Cosmic Ray Excess From Multi-Component Dark Matter Da Huang Physics Department, NTHU @ LeCosPA PRD89, 055021(2014) [arxiv: 1312.0366] PRD91, 095006 (2015) [arxiv: 1411.4450] Mod. Phys. Lett. A 30 (2015) 35, 1550188 In collaboration with C.-Q. Geng, L.-H. Tsai and C. Lai 1
Content Motivation and Review of Experimental Status General Phenomenological Analysis Two- Component Decaying DM Diffuse γ-ray Prediction Summary 2
Motivation Recently, AMS-02 published a series of new measurements of the positron fraction spectrum, showing an uprise above 10 GeV. AMS-02 Positron Fraction Spectrum Confirm the observation by many previous experiments, such as PAMELA, Fermi-LAT, AMS- 01, et al.. Different from usual astrophysical expection: decreasing power law 3
Motivation The excess was also observed in the total e + +e - flux spectrum by PAMELA, Fermi-LAT and AMS-02. Femi-LAT e + +e - Spectrum Conventional expectation: decreasing power law 4
Motivation Moreover, both the AMS-02 positron fraction spectrum and the Femi-LAT total e + +e - flux spectrum showed some substructure around 100 GeV. AMS-02 Positron Fraction Spectrum Femi-LAT e + +e - Spectrum Substructure? 5
Motivation In the new release, AMS-02 also gave the spectra of e + (e - ) flux and total (e + +e - ) flux. e + (e - ) flux: Spectrum hardening above ~30 GeV 6
Motivation Positron fraction : first evidence that positron fraction stops increasing with energy above ~200 GeV Total e + +e - flux: good fit with a single power law at high energy AMS-02 Positron Fraction Spectrum AMS-02 Spectrum of (e + +e - ) flux 7
Motivation All the excesses indicate that there are additional positron and/or electron sources beyond our current knowledge, either in astrophysical or particle physical origin. In literature, there are two compelling candidate origin for these excesses: Pulsars and Dark Matter. In this talk, I concentrate on the decaying dark matter interpretation for this AMS-02/Fermi-LAT excess Requirement the TeV DM lifetime τ DM ~O(10 26 )s >> τ Universe ~ O(10 17 )s 8
Decaying DM: Status Previous Studies concentrated on the Single-Component Decaying DM models with the dominant decay channels e + e -, μ + μ -, τ + τ -,W + W -, b + b -, Their general conclusion is that such models cannot explain the AMS-02 positron fraction and Fermi-LAT total e + +e - flux simultaneously. Jin et al APJ (2013) arxiv: 1304.1997; Yuan, et.al. arxiv: 1304.1482 Multi-Component DM 9
Further Constraints on Decaying DM The measured antiproton spectrum agrees with the prediction of the conventional astrophysical theory well 10
Further Constraints on Decaying DM Recent analysis with the new AMS-02 data confirmed this conclusion. Giesen et al ICAP(2015); Iin et al. PRD (2015); Kappl et al JCAP(2015). Leptophilic DM 11
Decaying DM: General Formula e - (e + ) flux: Primary electron flux: assumed to be broken power law Br = : Secondary e - (e + ) produced in propagation, computed by GALPROP κ 1,2 denotes the uncertainty in normalization of backgrounds. 12
Two-Component Decaying DM DM Source Term: ρ(x): DM density distribution, here we use isothermal profile τ i : DM lifetime M i : DM Mass Half Density DM decay process : DM Injection Spectra: with condition: 13
Two-Component Decaying DM Normalized Injection Spectra for Electrons : : obtained with the simulation by PYTHIA After e + /e - are produced from DM decays, they would propagate in the Galaxy, which is solved numerically by GALPROP 14
Two-Component Decaying DM Observations: The excess of total e + +e - flux by Fermi-LAT extends to 1 TeV, so at least one DM cutoff should be larger than 1 TeV; The substructure at around 100 GeV observed by both AMS-02 and Fermi-LAT AMS-02 Positron Fraction Spectrum Femi-LAT e + +e - Spectrum One DM drop at 100GeV Substructure? 15
Two-Component Decaying DM The observations above indicates that DM at least contains two components, with E c1 > 1000 GeV and E c2 100 GeV. For generic discussion, we take two DMs cutoffs E ci and masses M i as follows: E c1 M 1 E c2 M 2 1500 GeV 3030 GeV 100 GeV 416 GeV 16
Two-Component Decaying DM Fitting Results: Conclusion: Double-Component DM decaying mainly via two-body leptonic decay CAN fit to AMS-02 positron fraction and Fermi-LAT total Talk @ 2nd flux LeCosPA simultaneously. 17
Update with New AMS-02 Data Recently, we update our analysis of two-component decaying DM model with the AMS-02 positron fraction and total (e + +e - ) flux. C. Lai, DH, C. Q. Geng, MPLA 30 (2015) 35, 1550188 Advantage: reduce the systematic uncertainties of fit 18
Update with New AMS-02 Data Total e + +e - Flux Positron Fraction Spectrum All the cases fit the AMS-02 dataset very well. 19
Diffuse γ-ray Constraint Previous studies showed that the diffuse γ-ray measured by Fermi-LAT could already give strong constraint to decaying DM Cirelli et al PRD(2012); Essig et al. PRD (2009); Ibe et al(2013), 1305.0084; Cirelli & Panci, NPB (2009); Question: Does our two-component DM (or multi-component DM) scenario still survive after the consideration of diffuse γ-ray constraints? Strategy: We compute total various diffuse γ-ray spectrum, including the ones from two-component DM decays, which is compared with the Fermi-LAT data. Total Predictions of Phen. Model! 20
Model Prediction to Diffuse γ-ray Substructure? Conclusion: With the parameters fitted by AMS-02 and Fermi- LAT, the predicted γ ray is still allowed by the Fermi-LAT measurement. 21
Summary In this talk we investigate the multi-component decaying Dark Matter model to explain AMS-02 and Fermi-LAT e + /e - excesses, and show that two DM components are enough to explain the data. We also use the AMS-02 2014 data to update our analysis of two-component DM model, and show that it can also provide a good fit. We also show that the predicted diffuse γ-ray spectrum agrees with that observed by Fermi-LAT. 22
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Single-Component Decaying DM Χ 2 Fitting Results: 24
Update with New AMS-02 Data Total e + +e - Flux Positron Fraction Spectrum All the cases fit the AMS-02 data very well 2DM alive Observation: if E ch < 1 TeV, the positron fraction begins decreasing at ~200 GeV, as claimed by AMS-02, but it cannot explain the total (e + +e - ) flux at high energies. 25
Propagation Parameters 26